For decades, the agglomeration of comets from clathrates has been regularly invoked to explain their compositional and thermodynamic properties [1]}, [2]}, [3]}, [4]}, [5]}, [6]}. Recent measurements of 67P/C-G's composition by the Rosina mass spectrometer aboard the Rosetta mission have also been interpreted in favor of the presence of clathrates in its interior [7]}, [8]}, [9]}. This possibility is now investigated in the case of R2, which presents unusually high CO and N\(_2\)  abundances in its coma, compared to typical comets. To do so, we aim at comparing the plausible composition of multiple guest (MG) clathrates formed in the PSN to that of R2, assuming this latter would have agglomerated from these icy structures. These MG clathrates are assumed to be formed from a gaseous mixture composed of N\(_2\)  and CO, assuming these species are the two main C– and N–bearing volatiles in the gas phase of the disk, a hypothesis consistent with the thermochemical models [10]}, [11]}, [12]}. Because CO has a much higher propensity for clathration than N\(_2\) , the calculations utilized in this work are those performed in the framework of structure I clathrates, namely the structure predicted for a CO–dominated clathrate [13]}. Given the fact that half of protosolar carbon is expected to be used in organic compounds in the PSN [14]}, only the remaining half is assumed to be in the form of CO. Assuming that 90% of protosolar nitrogen is in N\(_2\)  form [10]}, we derive a N\(_2\) /CO ratio of 2.66 \(\times \)  10\(^{-1}\)  in the initial gas phase of the PSN, based on the protosolar abundances given by [16]}. In our model, clathrates form in the PSN as long as crystalline water is available. Here we assume that once all the water budget has been used for clathration, the remaining volatiles are not incorporated into solids.
